/ftp/cats/A+A/591/A11



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J/A+A/591/A11       SMC BV photometry of 9 star cluster fields    (Dias+, 2016)
The following files can be converted to FITS (extension .fit or fit.gz)
	table2.dat b*.dat h*.dat k*.dat lind14.dat ngc152.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/591/A11
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drwxr-xr-x 36 cats archive 4096 Oct 24 2016 [Up] drwxr-xr-x 3 cats archive 4096 Jan 12 2023 [TAR file] -rw-r--r-- 1 cats archive 510 Dec 19 2022 .message -r--r--r-- 1 cats archive 8131 Jun 3 2016 ReadMe -rw-r--r-- 1 cats archive 1010 Jun 3 2016 +footg5.gif -rw-r--r-- 1 cats archive 3007 Jun 3 2016 +footg8.gif -r--r--r-- 1 cats archive 48564 May 13 2016 bruck2.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 103170 May 13 2016 bruck4.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 94563 May 13 2016 bruck6.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 145977 May 13 2016 hw5.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 167694 May 13 2016 hw6.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 68970 May 13 2016 kron11.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 213408 May 13 2016 kron8.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 157434 May 13 2016 lind14.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 170943 May 13 2016 ngc152.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 812 May 17 2016 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/A+A/591/A11 SMC BV photometry of 9 star cluster fields (Dias+, 2016) ================================================================================ SMC west halo: a slice of the galaxy that is being tidally stripped? Star clusters trace age and metallicity gradients. Dias B., Kerber L., Barbuy B., Bica E., Ortolani S. <Astron. Astrophys. 591, A11 (2016)> =2016A&A...591A..11D (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Magellanic Clouds ; Clusters, open ; Clusters, globular ; Photometry, CCD ; Photometry, UBV Keywords: galaxies: star clusters - Magellanic Clouds - galaxies: structure - Hertzsprung-Russell (HR) and C-M diagrams - galaxies: stellar content Abstract: The evolution and structure of the Magellanic Clouds is currently under debate. The classical scenario in which both the Large and Small Magellanic Clouds (LMC, SMC) are orbiting the Milky Way has been challenged by an alternative in which the LMC and SMC are in their first close passage to our Galaxy. The clouds are close enough to us to allow spatially resolved observation of their stars, and detailed studies of stellar populations in the galaxies are expected to be able to constrain the proposed scenarios. In particular, the west halo (WH) of the SMC was recently characterized with radial trends in age and metallicity that indicate tidal disruption. We intend to increase the sample of star clusters in the west halo of the SMC with homogeneous age, metallicity, and distance derivations to allow a better determination of age and metallicity gradients in this region. Distances and positions are compared with the orbital plane of the SMC depending on the scenario adopted. Comparisons of observed and synthetic V(B-V) colour-magnitude diagrams were used to derive age, metallicity, distance, and reddening for star clusters in the SMC west halo. Observations were carried out using the 4.1m SOAR telescope. Photometric completeness was determined through artificial star tests, and the members were selected by statistical comparison with a control field. We derived an age of 1.23+/-0.07Gyr and [Fe/H]=-0.87+/-0.07 for the reference cluster NGC 152, compatible with literature parameters. Age and metallicity gradients are confirmed in the WH: 2.6+/-0.6Gyr/deg and -0.19+/-0.09dex/deg, respectively. The age-metallicity relation for the WH has a low dispersion in metallicity and is compatible with a burst model of chemical enrichment. All WH clusters seem to follow the same stellar distribution predicted by dynamical models, with the exception of AM-3, which should belong to the counter-bridge. Bruck 6 is the youngest cluster in our sample. It is only 130+/-40Myr old and may have been formed during the tidal interaction of SMC-LMC that created the WH and the Magellanic bridge. We suggest that it is crucial to split the SMC cluster population into groups: main body, wing and bridge, counter-bridge, and WH. This is the way to analyse the complex star formation and dynamical history of our neighbour. In particular, we show that the WH has clear age and metallicity gradients and an age-metallicity relation that is also compatible with the dynamical model that claims a tidal influence of the LMC on the SMC. Description: Photometric magnitudes from SOAR Optical Imager for individual stars in nine stellar clusters in the Small Magellanic Cloud are presented. The following clusters are presented: Bruck2, Bruck4, Bruck6, HW5, HW6, Kron8, Kron11, Lindsay14, and NGC152. For each star equatorial coordinates and B, V (Bessel) magnitudes with their errors are given.